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KAKEN_15K05026seika.pdf
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:304.3 KB
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:Oct 31, 2019 |
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Total downloads since Oct 31, 2019 : 380
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新星からIa型超新星へ : 連星系理論の精密化
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シンセイ カラ Iaガタ チョウシンセイ エ : レンセイケイ リロン ノ セイミツカ
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Shinsei kara Iagata chōshinsei e : renseikei riron no seimitsuka
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From nova to type Ia supernova : toward sophisticated binary evolution
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加藤, 万里子
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カトウ, マリコ
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Katō, Mariko
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慶應義塾大学・理工学部 (日吉) ・教授
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Research team head
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科研費研究者番号 : 50185873
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2019
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科学研究費補助金研究成果報告書
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2018
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新星の光度曲線は加藤の新星風理論で記述できる。これに基づき光度曲線解析の手法を独自に開発し、多数の新星の白色矮星の質量等を求めた。また色等級図上の進化には共通点があることを発見し、それを用いて距離と星間吸収を求めた。回帰新星 M31N 2008-12a(Ia型超新星の親天体候補）の毎年の爆発を国際共同観測で詳細に解析した。また質量が増加している白色矮星は、定期的にヘリウム核燃焼による爆発をおこし、そのさいシリコンなどの重元素が合成される。このような天体が超新星爆発をおこすと、爆発の初期に観測される高速吸収線が説明できることを理論的に示した。
The decay phase of nova outbursts can be followed by Kato's optically thick wind theory. Based on this method, we analyzed a number of nova light curves to determine binary parameters such as the white dwarf mass. We proposed stretched color-magnitude diagram and found common paths. Using this property we determined the distance and interstellar absorption of each nova. The recurrent nova M31N 2008-12a, a most promising candidate of Type Ia supernova, is observed in detail by our international observation team and I contributed from the theoretical side. We also calculated silicon and heavy element production during He shell flash on very massive white dwarfs that explains high velocity feature commonly observed in early phase of SN Ia explosion.
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研究種目 : 基盤研究 (C) (一般)
研究期間 : 2015～2018
課題番号 : 15K05026
研究分野 : 天文学
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